Figure 18 from The Next Generation Virgo Cluster Survey (NGVS). I. Introduction to the Survey

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The Next Generation Virgo Cluster Survey (NGVS). I. Introduction to the Survey

Authors: Laura Ferrarese, Patrick Côté, Jean-Charles Cuillandre, S. D. J. Gwyn, Eric W. Peng, Lauren A. MacArthur, Pierre-Alain Duc, A. Boselli, Simona Mei, Thomas Erben, Alan W. McConnachie, Patrick R. Durrell, J. Christopher Mihos, Andrés Jordán, Ariane Lançon, Thomas H. Puzia, Eric Emsellem, Michael L. Balogh, John P. Blakeslee, Ludovic van Waerbeke, Raphaël Gavazzi, Bernd Vollmer, J. J. Kavelaars, David Woods, Nicholas M. Ball, S. Boissier, Stéphane Courteau, E. Ferriere, G. Gavazzi, Hendrik Hildebrandt, P. Hudelot, M. Huertas-Company, Chengze Liu, Dean McLaughlin, Y. Mellier, Martha Milkeraitis, David Schade, Chantal Balkowski, Frédéric Bournaud, R. G. Carlberg, S. C. Chapman, Henk Hoekstra, Chien Peng, Marcin Sawicki, Luc Simard, James E. Taylor, R. Brent Tully, Wim van Driel, Christine D. Wilson, Todd Burdullis, Billy Mahoney, and Nadine Manset

Ferrarese et al. 2012 The Astrophysical Journal Supplement Series 200 4.

Provider: AAS Journals

Caption: Figure 18.

Azimuthally averaged major-axis surface brightness profile of M49, the first-ranked member of the Virgo cluster, from the NGVS (black circles) compared to various profiles from the literature (as indicated in the lower left corner). Profiles have been shifted into the g band for comparison to the NGVS data by applying a constant color offset measured in the range 10''–30''. The smooth curve shows a "core-Sérsic" model (Graham et al. 2003) fitted to the NGVS profile (which reaches ~3000'', or 240 kpc, along the major axis) after combining with the HST profile from Ferrarese et al. (2006a; red circles). Vertical marks indicate the radii containing different percentages of the galaxy luminosity according to the fitted model.

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